TY - JOUR
T1 - The Simons Observatory
T2 - Magnetic Sensitivity Measurements of Microwave SQUID Multiplexers
AU - Vavagiakis, Eve M.
AU - Ahmed, Zeeshan
AU - Ali, Aamir
AU - Arnold, Kam
AU - Austermann, Jason
AU - Bruno, Sarah Marie
AU - Choi, Steve K.
AU - Connors, Jake
AU - Cothard, Nicholas
AU - Dicker, Simon
AU - Dober, Brad
AU - Duff, Shannon
AU - Fanfani, Valentina
AU - Healy, Erin
AU - Henderson, Shawn
AU - Ho, Shuay Pwu Patty
AU - Hoang, Duc Thuong
AU - Hilton, Gene
AU - Hubmayr, Johannes
AU - Krachmalnicoff, Nicoletta
AU - Li, Yaqiong
AU - Mates, John
AU - McCarrick, Heather
AU - Nati, Federico
AU - Niemack, Michael
AU - Silva-Feaver, Maximiliano
AU - Staggs, Suzanne
AU - Stevens, Jason
AU - Vissers, Mike
AU - Ullom, Joel
AU - Wagoner, Kasey
AU - Xu, Zhilei
AU - Zhu, Ningfeng
N1 - Publisher Copyright:
© 2002-2011 IEEE.
PY - 2021/8
Y1 - 2021/8
N2 - The Simons Observatory (SO) will be a cosmic microwave background (CMB) survey experiment with three small-aperture telescopes and one large-aperture telescope, which will observe from the Atacama Desert in Chile. In total, SO will field $\sim$70,000 transition-edge sensor (TES) bolometers in six spectral bands centered between 27 and 280 GHz in order to achieve the sensitivity necessary to measure or constrain numerous cosmological quantities. The SO Universal Focal Plane Modules (UFMs) each contain a 150 mm diameter TES detector array, horn or lenslet optical coupling, cold readout components, and magnetic shielding. SO will use a microwave SQUID multiplexing ($\mu$MUX) readout at an initial multiplexing factor of $\sim$1000; the cold (100 mK) readout components are packaged in a $\mu$MUX readout module, which is part of the UFM, and can also be characterized independently. The 100 mK stage TES bolometer arrays and microwave SQUIDs are sensitive to magnetic fields, and their measured response will vary with the degree to which they are magnetically shielded. We present measurements of the magnetic pickup of test microwave SQUID multiplexers as a study of various shielding configurations for the Simons Observatory. We discuss how these measurements motivated the material choice and design of the UFM magnetic shielding.
AB - The Simons Observatory (SO) will be a cosmic microwave background (CMB) survey experiment with three small-aperture telescopes and one large-aperture telescope, which will observe from the Atacama Desert in Chile. In total, SO will field $\sim$70,000 transition-edge sensor (TES) bolometers in six spectral bands centered between 27 and 280 GHz in order to achieve the sensitivity necessary to measure or constrain numerous cosmological quantities. The SO Universal Focal Plane Modules (UFMs) each contain a 150 mm diameter TES detector array, horn or lenslet optical coupling, cold readout components, and magnetic shielding. SO will use a microwave SQUID multiplexing ($\mu$MUX) readout at an initial multiplexing factor of $\sim$1000; the cold (100 mK) readout components are packaged in a $\mu$MUX readout module, which is part of the UFM, and can also be characterized independently. The 100 mK stage TES bolometer arrays and microwave SQUIDs are sensitive to magnetic fields, and their measured response will vary with the degree to which they are magnetically shielded. We present measurements of the magnetic pickup of test microwave SQUID multiplexers as a study of various shielding configurations for the Simons Observatory. We discuss how these measurements motivated the material choice and design of the UFM magnetic shielding.
KW - Magnetic field dependence
KW - SQUIDs
KW - microwave multiplexing
KW - supercondcuting detectors
UR - http://www.scopus.com/inward/record.url?scp=85103775884&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85103775884&partnerID=8YFLogxK
U2 - 10.1109/TASC.2021.3069294
DO - 10.1109/TASC.2021.3069294
M3 - Article
AN - SCOPUS:85103775884
SN - 1051-8223
VL - 31
JO - IEEE Transactions on Applied Superconductivity
JF - IEEE Transactions on Applied Superconductivity
IS - 5
M1 - 9388904
ER -